2019A&A...623A...2A


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.24CET01:23:11

2019A&A...623A...2A - Astronomy and Astrophysics, volume 623A, 2-2 (2019/3-1)

Complex gamma-ray behavior of the radio galaxy M 87.

AIT BENKHALI F., CHAKRABORTY N. and RIEGER F.M.

Abstract (from CDS):


Context. In recent years, non-blazar active galactic nuclei (AGN) such as radio galaxies have emerged as a highly instructive source class providing unique insights into high energy acceleration and radiation mechanisms.
Aims. Here we aim to produce a detailed characterization of the high-energy (HE; >100MeV) gamma-ray emission from the prominent radio galaxy M 87.
Methods. We analyzed approximately eight years of Fermi-LAT data and derived the spectral energy distribution between 100MeV and 300GeV. We extracted lightcurves and investigated the variability behavior for the entire energy range as well as below and above 10GeV.
Results. Our analysis provides (i) evidence for HE gamma-ray flux variability and (ii) indications for a possible excess over the standard power-law model above Eb∼10GeV, similar to the earlier indications in the case of Cen A. When viewed in HE-VHE context, this is most naturally explained by an additional component dominating the highest-energy part of the spectrum. Investigation of the γ-ray lightcurves suggests that the lower-energy (<10GeV) component is variable on timescales of (at least) a few months. The statistics of the high energy component (>10GeV) does not allow significant constraints on variability. We do, however, find indications for spectral changes with time that support variability of the putative additional component and seem to favor jet-related scenarios for its origin capable of accommodating month-type variability.
Conclusions. The current findings suggest that both the high-energy (>Eb) and the very high energy (VHE; >100GeV) emission in M 87 are compatible with originating from the same physical component. The variability behavior at VHE then allows further constraints on the location and the nature of the second component. In particular, these considerations suggest that the VHE emission during the quiescent state originates in a similar region as during the flare.

Abstract Copyright: © ESO 2019

Journal keyword(s): radiation mechanisms: non-thermal - galaxies: active - gamma rays: galaxies - galaxies: jets - galaxies: elliptical and lenticular, cD - galaxies: individual: M 87

Simbad objects: 6

goto Full paper

goto View the reference in ADS

Number of rows : 6

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 4C 21.35 QSO 12 24 54.4583467193 +21 22 46.385219365   17.56 17.50 18.2   ~ 577 2
2 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5952 0
3 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5389 1
4 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6322 3
5 [VV2006] J123932.7+044305 QSO 12 39 32.7556681 +04 43 05.233027   20.81 20.56 18.1   ~ 131 2
6 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 4055 3

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2019A&A...623A...2A and select 'bookmark this link' or equivalent in the popup menu


2021.01.24-01:23:11

© Université de Strasbourg/CNRS

    • Contact